--- title: Supergiant summary: A massive star in a late stage of life, tens of thousands to hundreds of thousands of times as luminous as the Sun, of luminosity class I. Red supergiants such as Betelgeuse are among the largest stars known; blue ones such as Rigel are among the brightest. Most end as supernovae within a few million years of forming. science_status: [observed, model, sim] categories: [Stars, Supergiant stars, Stellar evolution, Massive stars] aliases: [Supergiants, Supergiant star, Red supergiant, Red supergiants, Blue supergiant, Blue supergiants, Yellow supergiant, Hypergiant, Hypergiants, Luminosity class I, Ia supergiant, RSP, BSP, Humphreys-Davidson limit, Red supergiant problem, Siwarha, Betelgeuse B] infobox: type: star_class name: Supergiant image: File:Betelgeuse_Great_Dimming_ESO_eso2109a.jpg caption: "Observation: Betelgeuse before and during its Great Dimming of 2019 to 2020, imaged with ESO's Very Large Telescope. Credit: ESO/M. Montargès et al." code: "BSP, BWP, WSP, YWP, YSP, OGP, RSP (blue to red supergiants); hypergiant classes defined but unused" stellar_class_key: "blue_supergiant to red_supergiant (seven colours)" spectral_types_covered: "O to M" luminosity_class: "Ia, Iab, Ib (supergiants); 0 or Ia+ (hypergiants)" effective_temperature: {value: "about 3,400 (red) to above 20,000 (blue)", unit: K, source: observed} mass: {value: "about 8 to several tens (initial)", unit: M_Sun, source: model} radius: {value: "tens (blue) to about 1,500 (red)", unit: R_Sun, source: observed} luminosity: {value: "about 10,000 to about 500,000", unit: L_Sun, source: observed} main_sequence_lifetime: {value: "a few million to a few tens of millions of years in all; the supergiant phase is the last tenth or so", unit: yr, source: model} perceived_colour: "From blue-white (Rigel, Deneb) to deep orange (Betelgeuse, Antares)" activity: "Strong winds and mass loss; pulsations; giant convection cells; episodic mass ejections" share_of_stars: "Tiny: none within 10 pc; about 5,000 of the 119,626 stars in the game's catalogue, because they are visible from far away" planet_occurrence: "No confirmed planets around supergiants" subtypes: "Blue, blue-white, white, yellow-white, yellow, orange and red supergiants (sim classes by spectral letter)" real_examples: "Betelgeuse (M1-M2Ia-Iab), Antares (M1.5Iab), Rigel (B8Ia), Deneb (A2Ia), Polaris (F8Ib), VY Canis Majoris, WOH G64" physics_engine: "Supergiant physics engines and subtype classifiers; measured overrides for named stars" science_doc: "The sim's supergiant science references" last_verified: "2026-09-27, writer B" sim: entity: stellar_class.supergiant refs: - id: joyce20 type: article-journal author: [{family: Joyce, given: Meridith}, {family: Leung, given: Shing-Chi}, {family: Molnár, given: László}, {literal: "et al."}] title: "Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA" container-title: The Astrophysical Journal volume: 902 page: 63 issued: 2020 DOI: 10.3847/1538-4357/abb8db - id: montarges21 type: article-journal author: [{family: Montargès, given: M.}, {family: Cannon, given: E.}, {family: Lagadec, given: E.}, {literal: "et al."}] title: "A dusty veil shading Betelgeuse during its Great Dimming" container-title: Nature volume: 594 page: 365-368 issued: 2021 DOI: 10.1038/s41586-021-03546-8 - id: levesque20 type: article-journal author: [{family: Levesque, given: Emily M.}, {family: Massey, given: Philip}] title: "Betelgeuse Just Is Not That Cool: Effective Temperature Alone Cannot Explain the Recent Dimming of Betelgeuse" container-title: The Astrophysical Journal Letters volume: 891 page: L37 issued: 2020 DOI: 10.3847/2041-8213/ab7935 - id: dupree22 type: article-journal author: [{family: Dupree, given: Andrea K.}, {family: Strassmeier, given: Klaus G.}, {family: Calderwood, given: Thomas}, {literal: "et al."}] title: "The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences" container-title: The Astrophysical Journal volume: 936 page: 18 issued: 2022 DOI: 10.3847/1538-4357/ac7853 - id: goldberg24 type: article-journal author: [{family: Goldberg, given: Jared A.}, {family: Joyce, given: Meridith}, {family: Molnár, given: László}] title: "A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in alpha Orionis" container-title: The Astrophysical Journal volume: 977 page: 35 issued: 2024 DOI: 10.3847/1538-4357/ad87f4 - id: macleod25 type: article-journal author: [{family: MacLeod, given: Morgan}, {family: Blunt, given: Sarah}, {family: De Rosa, given: Robert J.}, {literal: "et al."}] title: "Radial Velocity and Astrometric Evidence for a Close Companion to Betelgeuse" container-title: The Astrophysical Journal volume: 978 page: 50 issued: 2025 DOI: 10.3847/1538-4357/ad93c8 - id: howell25 type: article-journal author: [{family: Howell, given: Steve B.}, {family: Ciardi, given: David R.}, {family: Clark, given: Catherine A.}, {literal: "et al."}] title: "The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse" container-title: The Astrophysical Journal Letters volume: 988 page: L47 issued: 2025 DOI: 10.3847/2041-8213/adeaaf - id: goldberg25 type: article-journal author: [{family: Goldberg, given: Jared A.}, {family: O'Grady, given: Anna J. G.}, {family: Joyce, given: Meridith}, {literal: "et al."}] title: "Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to alpha Orionis from HST" container-title: The Astrophysical Journal volume: 994 page: 101 issued: 2025 DOI: 10.3847/1538-4357/ae0c0c - id: montarges26 type: article-journal author: [{family: Montargès, given: M.}, {family: Boccaletti, given: A.}, {family: Flasseur, given: O.}, {literal: "et al."}] title: "VLT/SPHERE images of the candidate companion of Betelgeuse" container-title: Astronomy & Astrophysics volume: 711 page: L12 issued: 2026 DOI: 10.1051/0004-6361/202661023 - id: eso2611 type: webpage author: [{literal: "ESO"}] title: "Astronomers find strongest evidence yet that Betelgeuse has a companion (press release eso2611)" URL: https://www.eso.org/public/news/eso2611/ issued: 2026-07-28 accessed: 2026-09-27 - id: iaucsn type: dataset author: [{literal: "IAU Working Group on Star Names"}] title: "IAU Catalog of Star Names (Siwarha, alpha Orionis B, approved 2025-09-22)" URL: https://exopla.net/star-names/modern-iau-star-names/ accessed: 2026-09-27 - id: ohnaka13 type: article-journal author: [{family: Ohnaka, given: K.}, {family: Hofmann, given: K.-H.}, {family: Schertl, given: D.}, {literal: "et al."}] title: "High spectral resolution imaging of the dynamical atmosphere of the red supergiant Antares in the CO first overtone lines with VLTI/AMBER" container-title: Astronomy & Astrophysics volume: 555 page: A24 issued: 2013 DOI: 10.1051/0004-6361/201321063 - id: ohnaka17 type: article-journal author: [{family: Ohnaka, given: K.}, {family: Weigelt, given: G.}, {family: Hofmann, given: K.-H.}] title: "Vigorous atmospheric motion in the red supergiant star Antares" container-title: Nature volume: 548 page: 310-312 issued: 2017 DOI: 10.1038/nature23445 - id: moravveji12 type: article-journal author: [{family: Moravveji, given: Ehsan}, {family: Guinan, given: Edward F.}, {family: Shultz, given: Matt}, {literal: "et al."}] title: "Asteroseismology of the Nearby SN-II Progenitor: Rigel. I. The MOST High-precision Photometry and Radial Velocity Monitoring" container-title: The Astrophysical Journal volume: 747 page: 108 issued: 2012 DOI: 10.1088/0004-637X/747/2/108 - id: dealmeida22 type: article-journal author: [{family: de Almeida, given: E. S. G.}, {family: Hugbart, given: M.}, {family: Domiciano de Souza, given: A.}, {literal: "et al."}] title: "Combined spectroscopy and intensity interferometry to determine the distances of the blue supergiants P Cygni and Rigel" container-title: Monthly Notices of the Royal Astronomical Society volume: 515 page: 1-12 issued: 2022 DOI: 10.1093/mnras/stac1617 - id: schiller08 type: article-journal author: [{family: Schiller, given: F.}, {family: Przybilla, given: N.}] title: "Quantitative spectroscopy of Deneb" container-title: Astronomy & Astrophysics volume: 479 page: 849-858 issued: 2008 DOI: 10.1051/0004-6361:20078590 - id: evans24 type: article-journal author: [{family: Evans, given: Nancy Remage}, {family: Schaefer, given: Gail H.}, {family: Gallenne, given: Alexandre}, {literal: "et al."}] title: "The Orbit and Dynamical Mass of Polaris: Observations with the CHARA Array" container-title: The Astrophysical Journal volume: 971 page: 190 issued: 2024 DOI: 10.3847/1538-4357/ad5e7a - id: wittkowski12 type: article-journal author: [{family: Wittkowski, given: M.}, {family: Hauschildt, given: P. H.}, {family: Arroyo-Torres, given: B.}, {family: Marcaide, given: J. M.}] title: "Fundamental properties and atmospheric structure of the red supergiant VY Canis Majoris based on VLTI/AMBER spectro-interferometry" container-title: Astronomy & Astrophysics volume: 540 page: L12 issued: 2012 DOI: 10.1051/0004-6361/201219126 - id: zhang12 type: article-journal author: [{family: Zhang, given: B.}, {family: Reid, given: M. J.}, {family: Menten, given: K. M.}, {family: Zheng, given: X. W.}] title: "Distance and Kinematics of the Red Hypergiant VY CMa: Very Long Baseline Array and Very Large Array Astrometry" container-title: The Astrophysical Journal volume: 744 page: 23 issued: 2012 DOI: 10.1088/0004-637X/744/1/23 - id: ohnaka24 type: article-journal author: [{family: Ohnaka, given: K.}, {family: Hofmann, given: K.-H.}, {family: Weigelt, given: G.}, {literal: "et al."}] title: "Imaging the innermost circumstellar environment of the red supergiant WOH G64 in the Large Magellanic Cloud" container-title: Astronomy & Astrophysics volume: 691 page: L15 issued: 2024 DOI: 10.1051/0004-6361/202451820 - id: munozsanchez26 type: article-journal author: [{family: Muñoz-Sanchez, given: Gonzalo}, {family: Kalitsounaki, given: Maria}, {family: de Wit, given: Stephan}, {literal: "et al."}] title: "The dramatic transition of the extreme red supergiant WOH G64 to a yellow hypergiant" container-title: Nature Astronomy volume: 10 page: 702-713 issued: 2026 DOI: 10.1038/s41550-026-02789-7 - id: vanloon26 type: article-journal author: [{family: van Loon, given: Jacco Th.}, {family: Ohnaka, given: Keiichi}] title: "A phoenix rises from the ashes: WOH G64 is still a red supergiant, for now" container-title: Monthly Notices of the Royal Astronomical Society volume: 546 page: stag012 issued: 2026 DOI: 10.1093/mnras/stag012 - id: hd79 type: article-journal author: [{family: Humphreys, given: R. M.}, {family: Davidson, given: K.}] title: "Studies of luminous stars in nearby galaxies. III. Comments on the evolution of the most massive stars in the Milky Way and the Large Magellanic Cloud" container-title: The Astrophysical Journal volume: 232 page: 409 issued: 1979 DOI: 10.1086/157301 - id: davies18 type: article-journal author: [{family: Davies, given: Ben}, {family: Crowther, given: Paul A.}, {family: Beasor, given: Emma R.}] title: "The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys-Davidson limit revisited" container-title: Monthly Notices of the Royal Astronomical Society volume: 478 page: 3138-3148 issued: 2018 DOI: 10.1093/mnras/sty1302 - id: smartt09 type: article-journal author: [{family: Smartt, given: S. J.}, {family: Eldridge, given: J. J.}, {family: Crockett, given: R. M.}, {family: Maund, given: J. R.}] title: "The death of massive stars. I. Observational constraints on the progenitors of Type II-P supernovae" container-title: Monthly Notices of the Royal Astronomical Society volume: 395 page: 1409-1437 issued: 2009 DOI: 10.1111/j.1365-2966.2009.14506.x - id: smartt15 type: article-journal author: [{family: Smartt, given: S. J.}] title: "Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars" container-title: Publications of the Astronomical Society of Australia volume: 32 page: e016 issued: 2015 DOI: 10.1017/pasa.2015.17 - id: db20 type: article-journal author: [{family: Davies, given: Ben}, {family: Beasor, given: Emma R.}] title: "The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors" container-title: Monthly Notices of the Royal Astronomical Society volume: 493 page: 468-476 issued: 2020 DOI: 10.1093/mnras/staa174 - id: beasor25 type: article-journal author: [{family: Beasor, given: Emma R.}, {family: Smith, given: Nathan}, {family: Jencson, given: Jacob E.}] title: "The Red Supergiant Progenitor Luminosity Problem" container-title: The Astrophysical Journal volume: 979 page: 117 issued: 2025 DOI: 10.3847/1538-4357/ad8f3f - id: kilpatrick25 type: article-journal author: [{family: Kilpatrick, given: Charles D.}, {family: Suresh, given: Aswin}, {family: Davis, given: Kyle W.}, {literal: "et al."}] title: "The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star" container-title: The Astrophysical Journal Letters volume: 992 page: L10 issued: 2025 DOI: 10.3847/2041-8213/ae04de - id: heger03 type: article-journal author: [{family: Heger, given: A.}, {family: Fryer, given: C. L.}, {family: Woosley, given: S. E.}, {literal: "et al."}] title: "How Massive Single Stars End Their Life" container-title: The Astrophysical Journal volume: 591 page: 288-300 issued: 2003 DOI: 10.1086/375341 - id: dejager98 type: article-journal author: [{family: de Jager, given: Cornelis}] title: "The yellow hypergiants" container-title: Astronomy and Astrophysics Review volume: 8 page: 145-180 issued: 1998 DOI: 10.1007/s001590050009 images_wanted: - file: File:Betelgeuse_Great_Dimming_ESO_eso2109a.jpg subject: "Four VLT/SPHERE images of Betelgeuse's disc: January 2019 bright, then December 2019, January 2020 and March 2020 with the southern half dimmed" source: eso page_url: https://www.eso.org/public/images/eso2109a/ credit: "ESO/M. Montargès et al." licence: "CC BY 4.0 (ESO usage terms)" - file: File:Betelgeuse_companion_VLT_ESO_eso2611a.jpg subject: "VLT images of Betelgeuse and the faint point of light of its candidate companion close beside it" source: eso page_url: https://www.eso.org/public/images/eso2611a/ credit: "ESO/M. Montargès et al. Background: N. Rissinger (skysurvey.org)" licence: "CC BY 4.0 (ESO usage terms)" - file: File:Antares_surface_VLTI_ESO_eso1726a.jpg subject: "Reconstructed VLTI view of the surface of the red supergiant Antares, the first detailed map of motions in another star's atmosphere" source: eso page_url: https://www.eso.org/public/images/eso1726a/ credit: "ESO/K. Ohnaka" licence: "CC BY 4.0 (ESO usage terms)" - file: File:WOH_G64_VLTI_ESO_eso2417a.jpg subject: "VLTI image of the red supergiant WOH G64 in the Large Magellanic Cloud, an elongated glow of dust around the star" source: eso page_url: https://www.eso.org/public/images/eso2417a/ credit: "ESO/K. Ohnaka et al." licence: "CC BY 4.0 (ESO usage terms)" --- A **supergiant** is a massive star in a late stage of its life, so luminous that it is given its own luminosity class, I, in the MK system of stellar classification. Supergiants are born with at least about eight times the Sun's mass and shine with tens of thousands to hundreds of thousands of times its light. They span every spectral type: blue supergiants such as Rigel are hot and compact for their class, while red supergiants such as Betelgeuse and Antares are cool, swollen to hundreds or more than a thousand times the Sun's radius, and among the largest stars known. Their lives are short, a few million to a few tens of millions of years, and most end in core-collapse supernovae. ## Characteristics ### Classes and colours Supergiants are graded Ia (luminous), Iab and Ib (less luminous); the most extreme, with luminosity class 0 or Ia+, are **hypergiants**, such as the yellow hypergiants that lie near the upper edge of stellar brightness :cite[dejager98]. By temperature they run from blue (O and B types, above about 10,000 K) through white and yellow (A, F and G) to red (K and M, down to about 3,400 K). The spread is mostly one of size: a massive star keeps roughly the same luminosity as it moves across the Hertzsprung-Russell diagram after leaving the main sequence, so as its surface cools from blue to red its radius must grow by tens of times to radiate the same energy. ### How bright a star can be There is an upper boundary to the luminosity of cool supergiants. Humphreys and Davidson found in 1979 that stars cooler than about 15,000 K do not exceed a bolometric absolute magnitude of about -9.5 to -10, about 500,000 to 800,000 times the Sun's luminosity, and attributed the limit to mass loss that strips the most massive stars before they can become red supergiants :cite[hd79]. A modern census of the Magellanic Clouds places the limit for cool supergiants lower, at about 320,000 solar luminosities :cite[davies18]. ### Winds, cells and pulsations Red supergiants lose mass rapidly in slow, dusty winds, and their surfaces are dominated by a few enormous convection cells. Interferometric maps of Antares show turbulent gas rising and falling at up to 20 km/s in an atmosphere extending to about 1.7 times the star's radius :cite[ohnaka17]. Betelgeuse pulsates with a period of about 400 days :cite[joyce20]. Blue supergiants drive fast winds with the pressure of their own light. ## Betelgeuse Betelgeuse, the red supergiant at the shoulder of Orion, is the best-studied example. Combining its evolution, pulsations and hydrodynamics, Joyce et al. (2020) estimated a present mass of 16.5 to 19 solar masses, a radius of 764 solar radii and a distance of 168 parsecs (548 light years) :cite[joyce20]; other methods give distances up to about 220 parsecs :cite[montarges21], so its true size and luminosity remain uncertain by tens of per cent. It is burning helium in its core and is expected to explode as a supernova, probably not for about a hundred thousand years :cite[joyce20]. Between late 2019 and early 2020 Betelgeuse faded by more than a magnitude, its **Great Dimming**. Images from the Very Large Telescope showed the southern half of the star darkened about tenfold, explained by a cloud of dust that formed over a cooler patch of the surface :cite[montarges21]; the star's temperature fell too little to explain the fading on its own :cite[levesque20]. Ultraviolet and optical spectra point to a large surface mass ejection as the cause, after which the star's 400-day pulsation disappeared for more than two years :cite[dupree22]. ::figure{src="File:Betelgeuse_Great_Dimming_ESO_eso2109a.jpg" size=wide alt="Four images of Betelgeuse's disc from 2019 and 2020, the lower half growing darker in the later frames" caption="Observation: Betelgeuse's surface in January 2019 and during the Great Dimming of December 2019 to March 2020, imaged with the VLT's SPHERE instrument. Credit: ESO/M. Montargès et al."} ### A companion Betelgeuse also brightens and fades on a long secondary period of about 2,100 days. In 2024 and 2025 two teams argued that this is caused by a companion star orbiting just outside the supergiant, of about one solar mass or less :cite[goldberg24] :cite[macleod25]. A speckle-imaging search with the Gemini North telescope then reported a probable detection, 52 milliarcseconds from Betelgeuse and about six magnitudes fainter in blue light :cite[howell25], and the companion has been given the name Siwarha by the International Astronomical Union :cite[iaucsn]. The Hubble Space Telescope saw no ultraviolet light from it, which rules out certain kinds of companion :cite[goldberg25]. On 28 July 2026 ESO announced the strongest evidence yet: images from the VLT's SPHERE instrument taken on 6 December 2024 show a source at a separation of 52.3 milliarcseconds, detected at more than six standard deviations :cite[eso2611] :cite[montarges26]. If it is a young star of the same age as Betelgeuse, its brightness implies 2.6 to 3.1 solar masses, above the dynamical estimates, and the authors describe it as a candidate whose confirmation awaits a second epoch of observation :cite[montarges26]. ::figure{src="File:Betelgeuse_companion_VLT_ESO_eso2611a.jpg" size=medium alt="Betelgeuse's bright disc with a faint point of light beside it" caption="Observation: VLT/SPHERE images of Betelgeuse and its candidate companion, released in July 2026. Credit: ESO/M. Montargès et al. Background: N. Rissinger (skysurvey.org)."} ## Other notable supergiants | Star | Type | Distance | Notes | |---|---|---|---| | Betelgeuse | M1-M2Ia-Iab | 168 to 220 pc | 764 solar radii, 16.5 to 19 solar masses; candidate companion :cite[joyce20] :cite[montarges26] | | Antares | M1.5Iab | about 170 pc | 680 solar radii (3.2 AU), 3,660 K :cite[ohnaka13] | | Rigel | B8Ia | about 260 pc | About 120,000 solar luminosities; a nearby future supernova :cite[dealmeida22] :cite[moravveji12] | | Deneb | A2Ia | uncertain | 8,525 K; about 200,000 solar luminosities if at the larger distance estimates :cite[schiller08] | | Polaris | F8Ib | | Pole Star; a pulsating Cepheid of 5.1 solar masses in a 30-year binary orbit :cite[evans24] | | VY Canis Majoris | M5Iae | 1.2 kpc | About 1,420 solar radii, among the largest stars known :cite[wittkowski12] :cite[zhang12] | | WOH G64 | red supergiant (LMC) | 50 kpc | First close-up image of a star in another galaxy :cite[ohnaka24] | WOH G64, in the Large Magellanic Cloud, shows how fast a supergiant can change. After the VLT Interferometer produced the first close-up image of a star outside the Milky Way in 2024 :cite[ohnaka24], one team reported that its spectrum had changed between 2013 and 2014 from a red supergiant's to that of a hotter yellow hypergiant :cite[munozsanchez26], while another found titanium oxide bands, the signature of a red supergiant, at every epoch from late 2024 to 2025 and argued that it may never have stopped being one :cite[vanloon26]. The question is open. ## The end of a supergiant Stars above about eight solar masses end with a collapsing iron core. Red supergiants are the progenitors of the commonest core-collapse supernovae, Type II-P; blue and yellow supergiants and stripped stars make other kinds; and the most massive may collapse to black holes, with or without an explosion :cite[heger03]. Archival images of exploded stars show that the progenitors of Type II-P supernovae range from about 8.5 to 16.5 solar masses, while red supergiants exist up to about 25: the **red supergiant problem** :cite[smartt09]. One explanation is that the heaviest red supergiants collapse to black holes without a visible supernova :cite[smartt15]. Others argue that the gap is not statistically significant once the uncertainties in progenitor brightness are included :cite[db20] :cite[beasor25]. The first supernova progenitor found with JWST, the star that became SN 2025pht in the galaxy NGC 1637, was a red supergiant of about 100,000 solar luminosities wrapped in carbon-rich dust :cite[kilpatrick25]. ::figure{src="File:Antares_surface_VLTI_ESO_eso1726a.jpg" size=medium alt="A reconstructed image of the red supergiant Antares showing a mottled disc" caption="Observation: the surface of Antares reconstructed from VLTI measurements, the first map of gas motions on another star. Credit: ESO/K. Ohnaka."} :::callout{type=sim title="In Pax Abyssi"} The sim assigns a star to a supergiant class whenever its catalogue spectral type carries luminosity class I, and names the class by the colour of its spectral letter, from blue (O) through blue-white, white, yellow-white, yellow and orange to red (M) supergiants. Hypergiant classes exist in the taxonomy but no catalogue star is assigned one yet. The game's catalogue holds about 5,000 real supergiants of every spectral type, K supergiants the largest group. Well-studied supergiants carry measured values in place of estimates from their colours: Betelgeuse is drawn at 764 solar radii, 3,600 K and 168 parsecs after Joyce et al. (2020), and Antares at 680 solar radii after Ohnaka et al. (2013). At the end of their lives the sim turns stars of 8 to 25 solar masses into neutron stars and heavier ones into black holes. ::: ## See also - [[Stellar classification]] - [[Red giant]] - [[Neutron star]] - [[Black hole]] - [[Wolf-Rayet star]] - [[Milky Way]]